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Title: The mass dependence of dwarf satellite galaxy quenching

Abstract

We combine observations of the Local Group with data from the NASA-Sloan Atlas to show the variation in the quenched fraction of satellite galaxies from low-mass dwarf spheroidals and dwarf irregulars to more massive dwarfs similar to the Magellanic Clouds. While almost all of the low-mass (M {sub *} ≲ 10{sup 7} M {sub ☉}) dwarfs are quenched, at higher masses the quenched fraction decreases to approximately 40%-50%. This change in the quenched fraction is large and suggests a sudden change in the effectiveness of quenching that correlates with satellite mass. We combine this observation with models of satellite infall and ram pressure stripping to show that the low-mass satellites must quench within 1-2 Gyr of pericenter passage to maintain a high quenched fraction, but that many more massive dwarfs must continue to form stars today even though they likely fell into their host >5 Gyr ago. We also characterize how the susceptibility of dwarfs to ram pressure must vary as a function of mass if it is to account for the change in quenched fractions. Though neither model predicts the quenching effectiveness a priori, this modeling illustrates the physical requirements that the observed quenched fractions place on possible quenchingmore » mechanisms.« less

Authors:
;  [1]
  1. Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States)
Publication Date:
OSTI Identifier:
22365080
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 792; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; EVOLUTION; MAGELLANIC CLOUDS; MASS; NASA; QUENCHING; SATELLITES; SIMULATION; STARS; STRIPPING; VARIATIONS

Citation Formats

Slater, Colin T., and Bell, Eric F., E-mail: ctslater@umich.edu, E-mail: ericbell@umich.edu. The mass dependence of dwarf satellite galaxy quenching. United States: N. p., 2014. Web. doi:10.1088/0004-637X/792/2/141.
Slater, Colin T., & Bell, Eric F., E-mail: ctslater@umich.edu, E-mail: ericbell@umich.edu. The mass dependence of dwarf satellite galaxy quenching. United States. doi:10.1088/0004-637X/792/2/141.
Slater, Colin T., and Bell, Eric F., E-mail: ctslater@umich.edu, E-mail: ericbell@umich.edu. Wed . "The mass dependence of dwarf satellite galaxy quenching". United States. doi:10.1088/0004-637X/792/2/141.
@article{osti_22365080,
title = {The mass dependence of dwarf satellite galaxy quenching},
author = {Slater, Colin T. and Bell, Eric F., E-mail: ctslater@umich.edu, E-mail: ericbell@umich.edu},
abstractNote = {We combine observations of the Local Group with data from the NASA-Sloan Atlas to show the variation in the quenched fraction of satellite galaxies from low-mass dwarf spheroidals and dwarf irregulars to more massive dwarfs similar to the Magellanic Clouds. While almost all of the low-mass (M {sub *} ≲ 10{sup 7} M {sub ☉}) dwarfs are quenched, at higher masses the quenched fraction decreases to approximately 40%-50%. This change in the quenched fraction is large and suggests a sudden change in the effectiveness of quenching that correlates with satellite mass. We combine this observation with models of satellite infall and ram pressure stripping to show that the low-mass satellites must quench within 1-2 Gyr of pericenter passage to maintain a high quenched fraction, but that many more massive dwarfs must continue to form stars today even though they likely fell into their host >5 Gyr ago. We also characterize how the susceptibility of dwarfs to ram pressure must vary as a function of mass if it is to account for the change in quenched fractions. Though neither model predicts the quenching effectiveness a priori, this modeling illustrates the physical requirements that the observed quenched fractions place on possible quenching mechanisms.},
doi = {10.1088/0004-637X/792/2/141},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 792,
place = {United States},
year = {2014},
month = {9}
}